Protoplanetary Disks
Protoplanetary disks are rotating circumstellar disks of gas and dust that surround young stars and are the birthplace of planets. These disks are formed from the leftover material that did not form the star and are typically composed of gas (mostly hydrogen and helium) and dust grains (silicates, carbon, and ice). The dust grains in the disk collide and stick together, eventually forming larger and larger bodies that can become planetesimals and eventually planets. Protoplanetary disks can vary in size and mass, with some extending out to hundreds of astronomical units from the central star. They are studied using a variety of techniques, including observations in the infrared, submillimeter, and radio wavelengths, as well as computer simulations. Understanding the properties and evolution of protoplanetary disks is crucial for understanding the formation and diversity of planetary systems.
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